Junfeng Wang, G. Fabbiano, G. Risaliti, M. Elvis, M. Karovska, A.
Zezas (Harvard-CfA/SAO), C. G. Mundell (Liverpool John Moores
University, UK), G. Dumas, E. Schinnerer (MPIA), J. M. Mazzarella,
J. H. Howell, and S. Lord (CalTech/IPAC)
Accretion Processes in X-Rays: From White Dwarfs to Quasars
07/13/2010
AGN outflow is an important
part of the accretion process
(cf. Proga, Chartas talks)
“AGN feedback” crucial to
SMBH-galaxy co-evolution
Energy injection efficiency
often assumed
Loutflow/Lbol ~ 5%-100%
(e.g., Scannapieco & Oh 2004;
Silk 2005; see also Hopkins & Elvis
2010; Ciotti et al. 2010; Ostriker et al.
2010)
Mrk 573
HST [OIII] survey by Schmitt et al. (2003); see also Bianchi et al. (2010)
Chandra contours
+ HST [OIII]
A single photoionized medium
- Overall morphology coincident
with the [OIII] emission
- Poor fit to the X-ray spectra with
collisionally ionized thermal
plasma
• Many Seyfert galaxies host
vigorous star formation and/or
eject relatively weak jets
NGC3393
Bianchi et al. (2006)
• Competing processes of AGN
photoionization and shock
heating
See also Evans et al. (2006); Bianchi et al. (2010); Dadina et al. (2010)
Blue: X-rays Red: [OIII]5007
[OIII] clouds P~10-10
dyne cm-2 (Kristen et al. 1997)
Pressure equilibrium
with cooler optical lineemitting gas
X-ray emitting hot gas
may serve as the hot
phase confining
inter-cloud medium to
the NLR cloud (Elvis et al.
1983, 1990)
Wang et al. (2009a)
1 kpc
Filled circles: NGC 1365 regions
Consistent with Type II SN
Diamond: Strickland (2004) starburst sample
Cyan circle and line: warm Galactic halo
enrichment
Blue squares: stellar yields from SNe Type I
Magenta squares: SNe Type II (Nakataki & Sato 1998 and references)
AGN Feedback Study: Spatial Resolution Needed
NGC 1068
Soft X-ray emission in Seyfert 2s likely dominated by photoionized gas
(Guainazzi & Bianchi 2007; Guainazzi et al. 2009) Line ratio diagnostics
But … location of the X-ray photoionized gas
e.g., Mrk 355 <0.06 pc (Longinotti+08); NGC 1068 up to 1 kpc (Evans+10) 
implications on the mass/momentum outflow
See Krongold+07; Arav+08; Steenbrugge+09; Ebrero+10
Biconical Outflow in NGC 4151 ENLR
Das et al. (2005)
Ogle et al. (2000); Yang et al. (2001)
~200 ks ACIS-S 1/8 sub-array
(shorter frametime)
-X-ray spectral variability of the
nucleus (Wang et al. 2010a)
-Extended soft X-ray emission
(Wang et al. 2010b)
NGC 4151
50 ks HRC-I Imaging the innermost region
(Wang et al. 2009)
0.13 arcsec `pixel’ but poor energy resolution
(cf. 0.5”/pixel ACIS)
1”
1”
65 pc
Wang et al. (2009); HST/FOC 502N data from Winge et al. (1997)
NGC 4151
Red: HRC 0.1-10 keV
Green: optical [OIII]
Blue: radio (1.4 GHz)
Wang J. et al. 2009, ApJ, 704, 1195
Ionization
parameter
ξ = L/(nr2)
n0(1pc)=103
Enhanced X-ray
emission
in addition to
photoionization
CLOUDY grid for an AGN photoionized medium (Bianchi et al. 2006) n rβ
Subpixel technique (Mori et al. 2001; Tsunemi et al. 2001; Kastner et al. 2002; Li et al. 2003)
HST [OIII]5007
0.1-1 keV
HRC PSF deconvolved
OVII
Contours: [OIII]
NeIX
Contours: 1.4 GHz
Ha: Knapen et al. (2004)
CO contours: Dumas et al.(2010)
Hardness ratio map of the
circum-nuclear region
reveal hard spectral index
or high obscuration region
Bianchi et al. (2008), Wang et al.
(2010)
inflow
outflow
Red: HI
Mundell et al. (1999)
Green: Halpha
Blue: 0.3-1 keV
X PSF scattering
X Unresolved point
sources
X Electron scattered
nuclear emission
Wang et al. (2010) ApJL submitted
? Relic photoionized gas from a past
AGN outburst (L~ Ledd required)
light travel time + recombination time scale
4
T < 2.5x10 yr
? Hot gas heated by AGN outflow
Pressure 10-11 dyne cm-2
Additional confinement by HI gas inflow
T~104 -105 yr
Chandra’s high resolution images are powerful tools in studying the
complex circum-nuclear regions of AGNs
 For the NGC 1365 X-ray emission cones, we find hot gas confining
photoionized clouds, likely starburst driven “superwind”
 In NGC 4151 Chandra resolves
o Photoionized emission. The radially constant ratio indicates a density
dependence n  r−2 as expected for a nuclear wind.
o Thermal emission from interaction between radio outflow and the NLR
clouds.
o ‘Fossil’ large scale emission.
Given these diversities, we need to study individual objects in detail to learn
AGN feedback physics
CHandra survey of Extended Emission line Regions in nearby Seyferts:
(CHEERS) Full picture of the multiphase ISM

Mass-momentum outflow
Subpixel technique
(Mori et al. 2001; Tsunemi et al. 2001; Kastner et al. 2002; Li et al. 2003)
applied
Wang et al. in prep.